The 24 \(\mu \) m image towards G11.36+0.80 (top middle panel in Fig. REF ) shows that there are dark absoprtion features to the south and south-east of clump B. The features are partly dark even at 70 \(\mu \) m, and this region is coincident with a weak (\(3\sigma \) ) protrusion-like feature in the LABOCA 870 \(\mu \) m image. These features could be subfilaments attached to G11.36+0.80. These types of subfilaments have been detected towards some other IRDCs as well (e.g. [1]}; [2]}; [3]}), and they are denser structures than the striations seen to be connected to some lower-mass filaments (e.g. [4]}; [5]}; [6]} and [7]} for recent reviews). The subfilaments seen towards G11.36+0.80 could be signatures of the filament formation through gas flows or gas accretion from the surrounding medium. However, high-resolution interferometric molecular line observations would be needed to test these hypotheses and the physical connection of the features with the main filament in the first place.
<TABLE>